Notes. The columns are: Miras’ name; the pulsation period P_obs obtained from light curves, its uncertainty is assumed to be 2.4% of the corresponding P_obs (Merchan-Benitez et al. 2023); RUWE; N_per the number of visibility periods used in the astrometric solution⁶, a visibility period consists of a group of observations separated from other groups by at least 4 days. A high number of periods is a indicator of a well-observed source while a value smaller than 10 indicates that the calculated parallax could be more vulnerable to errors (visibility_periods_used in the Gaia archive); N_good the total number of good observations along-scan (astrometric_n_good_obs_al) by Gaia to compute the astrometric solution; the luminosity L_★; the negative luminosity uncertainty $L_{\star }^{-}$; the positive luminosity uncertainty $L_{\star }^{+}$; the GDR3 parallax ϖ; the corrected GDR3 parallax ϖ_corr according to Lindegren et al. (2021); the parallax uncertainty population membership based on a study of stellar total space velocity according to Chen et al. (2021), halo stars are more metal poor.